High energy (X-ray) emission from HD 163296 · High energy (X-ray) emission from HD 163296 P....
Transcript of High energy (X-ray) emission from HD 163296 · High energy (X-ray) emission from HD 163296 P....
High energy (X-ray) emission from HD 163296
P. Christian Schneider
Hamburger Sternwarte
HAeBe stars workshopSantiago, Chile
April 7th, 2014
Overview
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FUV & optical emission from the jet(many photons)
X-ray emission from the jet(a few photons)
X-ray emission from the central component(some photons)
HD 163296
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spT: A2, Age: 4 MyrMontesinos et al. (2009)
d = 122 pc van Leeuwen 2007
No detected stellarmagnetic fieldHubrig et al. (2007), Wade et al. (2007),
Alecian et al. (2013)
log Maccr. ∼ −7Mendigutía et al. (2014), Ellerbroek et al.
(2014)
Well-known jet Devine et al.
(2000), Grady et al. (2000)
From Wassell et al. (2006)
The jet in Lyα and in optical lines
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STIS long-slit data from 2011: Mout ∼ 10−9M� yr−1
From Günther, Schneider & Li (2013)
. . . and from the jet!
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Adapted from Günther, Schneider & Li (2013)
From Güdel et al. (2011)
DG Tau
2003
2011
. . . and from the jet!
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Adapted from Günther, Schneider & Li (2013)
From Güdel et al. (2011)
DG Tau 2003
2011
. . . and from the jet!
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Adapted from Günther, Schneider & Li (2013)
From Güdel et al. (2011)
DG Tau
2003
2011
What does that mean?
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Highly significant detection(conf. 97% in 2003, 93% in 2011)
X-rays require T & 3× 106 K
translates to shock velocities of 500 km s−1
Evidence for high shock velocities?“classical” jet tracers indicate vs < 100 km s−1(e.g., Ellerbroek et al. 2014)
→ Look at Lyα
Lyα - Emission from forward & counter-jet
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Knot A
Knot B
Knot C
Air
glo
w
400 200 0 200 400Velocity (km s−1 )
10
8
6
4
2
0
2
4
6
8
10D
ista
nce
(arc
sec)
Knots?Knots?
1999
13.4
13.3
13.2
13.1
13.0
12.8
12.6
log(S
urf
ace
bri
ghtn
ess
) [e
rg s−
1 c
m−
2 a
rcse
c−2
−1]
Data from Devine et al. (2000)
Lyα - Emission from forward & counter-jet
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Knot A
Knot B
Knot C
Air
glo
w
400 200 0 200 400Velocity (km s−1 )
10
8
6
4
2
0
2
4
6
8
10D
ista
nce
(arc
sec)
Knots?Knots?
2000
13.4
13.3
13.2
13.1
13.0
12.8
12.6
log(S
urf
ace
bri
ghtn
ess
) [e
rg s−
1 c
m−
2 a
rcse
c−2
−1]
Data from Devine et al. (2000)
Lyα - Emission from forward & counter-jet
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Air
glo
w
400 200 0 200 400Velocity (km s−1 )
10
8
6
4
2
0
2
4
6
8
10D
ista
nce
(arc
sec)
Knots?Knots?
2011
13.4
13.3
13.2
13.1
13.0
12.8
12.6
log(S
urf
ace
bri
ghtn
ess
) [e
rg s−
1 c
m−
2 a
rcse
c−2
−1]
From Günther, Schneider & Li (2013)
X-ray vs. Lyα emission
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1213.0 1213.5 1214.0 1214.5 1215.0 1215.5Wavelength ( )
0.1
0.2
0.3
0.4
0.5Fl
ux (
a.u
.)
Air
glo
wv s f
or
X-r
ays
Lyα emission
600 500 400 300 200 100 0Projected velocity (km/s)
Adapted from Günther, Schneider & Li (2013)
Origin of the X-ray emission?
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Bulk velocities too low to explain X-rays
Minimum flow velocity required:ca. 600 km s−1 which implies a launching region closeto 0.1 AU for MHD disk winds
Possibility: Stationary shock at the base of the jet
Stellar X-ray properties of HD 163296
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log LX = 29.4Soft spectrum (mean energy 0.5 keV)O VII triplet → soft X-rays come & 2R? above thephotosphere (No signs of accretion)
From Günther & Schmitt (2009)
Non-stellar X-rays in YSOs
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Jet driving sources often show particular X-rayspectrum (TAX-sources, Güedel et al. 2007)Prime example: DG TauHowever, no offset in HD 163296 (X-rays within 30 AU)
0.1 0.0 0.1 0.2 0.3Offset (")
0.25
0.20
0.15
0.10
0.05
0.00
Off
set
(")
2004
2005
2006
2010
N
EDG Tau
Forward jet
direction
Centroid of the soft inner X-ray component
60
50
40
30
20
10
0
Dis
tance
(A
U)
Adapted from Schneider & Schmitt (2008)
Conclusions I
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Non-stellar, but “central” X-ray component
10 % of the jet mass loss required to powerX-ray emission (10−10 vs. 10−9M� yr−1)
X-ray properties similar to (some) CTTS→ X-rays related to innermost jet component→ Similar magnetic jet launching mechanism